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A Well-Balanced Unified Gas-Kinetic Scheme for Multiscale Flow Transport Under Gravitational Field

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A Well-Balanced Unified Gas-Kinetic Scheme for Multiscale Flow Transport Under Gravitational Field A Well-Balanced Unified Gas-Kinetic Scheme for Multiscale Flow Transport Under Gravitational Field Tianbai Xiaoa, Qingdong Caia, Kun Xub,∗ aDepartment of Mechanics and Engineering Science, College of Engineering, Peking University, Beijing 100871, China bDepartment of Mathematics, Department of Mechanical and Aerospace Engineering, Hong Kong University of Science and Technology, Clear Water Bay, Kowloon, Hong Kong Abstract The gas dynamics under gravitational field is usually associated with the multiple scale nature due to large density variation and a wide range of local Knudsen number. It is chal- lenging to construct a reliable numerical algorithm to accurately capture the non-equilibrium physical effect in different regimes. In this paper, a well-balanced unified gas-kinetic scheme (UGKS) for all flow regimes under gravitational field will be developed, which can be used for the study of non-equilibrium gravitational gas system. The well-balanced scheme here is defined as a method to evolve an isolated gravitational system under any initial condition to an isothermal hydrostatic equilibrium state and to keep such a solution. To preserve such a property is important for a numerical scheme, which can be used for the study of slowly evolving gravitational system, such as the formation of star and galaxy. Based on the Boltzmann model with external forcing term, an analytic time evolving (or scale-dependent) solution is constructed to provide the corresponding dynamics in the cell size and time step scale, which is subsequently used in the construction of UGKS. As a result, with the varia- tion of the ratio between the numerical time step and local particle collision time, the UGKS is able to recover flow physics in different regimes and provides a continuum spectrum of gas dynamics. For the first time, the flow physics of a gravitational system in the transition regime can be studied using the UGKS, and the non-equilibrium phenomena in such a grav- itational system can be clearly identified. Many numerical examples will be used to validate the scheme. New physical observation, such as the correlation between the gravitational field and the heat flux in the transition regime, will be presented. The current method provides an indispensable tool for the study of non-equilibrium gravitational system. Keywords: gravitational field, well-balanced property, unified gas-kinetic scheme, arXiv:1608.08730v1 [physics.comp-ph] 31 Aug 2016 multi-scale flow, non-equilibrium phenomena ∗Corresponding author Email addresses: [email protected] (Tianbai Xiao), [email protected] (Qingdong Cai), [email protected] (Kun Xu) Preprint submitted to Elsevier September 6, 2018 1. Introduction The universe is an evolving gravitational system. The gas dynamics due to the gravi- tational force plays a critical role in the star and galaxy formation, as well as atmospheric convection on the planets. For an evolving gravitational system, there is almost no any validated governing equation to describe the non-equilibrium dynamics uniformly across different regimes. The well-established statistical mechanics is mostly for the equilibrium solution. For an isolated gravitational system, under the conservation of mass, momentum, and energy, the system will eventually get to the isothermal equilibrium state from an arbi- trary initial condition. Such a steady-state solution will be maintained due to exact balance between the gravitational source term and the inhomogeneous flux function. For the study of a gravitational system, many numerical schemes have been developed. To capture such an equilibrium solution for an isolated gravitational system is a minimal requirement for a scheme which can be used in the astrophysical applications. The lack of well-balanced prop- erty may lead to spurious solution, or even present wrong physical solution for a long time evolving gravitational system. The purpose of this paper is to develop such a scheme which not only has the well-balanced property, but also be able to capture the non-equilibrium phenomena, which have not been studied theoretically or numerically for a gravitational system before. For the equilibrium flow, such as for the gravitational Euler system, many efforts have been devoted to the construction of well-balanced schemes. Leveque and Bale [1] developed a quasi-steady wave-propagation algorithm, which is able to capture perturbed quasi-steady solutions. Botta et al. [2] used local, time dependent hydrostatic reconstructions to achieve the hydrostatic balance. Xing and Shu [3] proposed a high-order WENO scheme to resolve small perturbations on the hydrostatic balance state on coarse meshes. The basic idea of these methods is to extend classical algorithm for the compressible Euler equations to the gravitational system with proper modifications. Different gas dynamic equations can be constructed under different modeling scales. In the kinetic scale, such as particle mean free path and traveling time between particle colli- sions, the Boltzmann equation is well established. In the hydrodynamic scale, even though the scale for its modeling is not clearly identified, the Euler and Navier-Stokes equations are routinely used. Due to the clear scale separation, both kinetic and hydrodynamic equations can be applied in their respective scales. However, the real gas dynamics may not have such a scale separation. With the scale variation between the kinetic and hydrodynamic ones, the gas dynamic equation should have a smooth transition from the Boltzmann to the Navier-Stokes equations. This multiple scale nature is especially important for a gravita- tional system, where due to the gravitational effect the density in the system can be varied largely, and so is the particle mean free path. With a fixed modeling scale, such as the mesh size in a numerical scheme, the cell’s Knudsen number Knc can be changed significantly. For a single gravitational system, the flow dynamics may vary from the kinetic Boltzmann modeling in the upper atmospheric layer to the hydrodynamic one in the inner high density region, with a continuous variation of flow physics. Therefore, a gravitational system has an intrinsic multiple scale nature. The corresponding numerical algorithm to simulate such a 2 system is preferable to have a property of providing a continuum spectrum of flow dynamics from rarefied to continuum one. In recent years, the unified gas-kinetic scheme has been developed for the simulation of multiple scale flow problems [4, 5, 6, 7]. This algorithm is based on the direct physical modeling on the mesh size scale, such as constructing the corresponding governing equations in such a scale. The scheme is able to capture physical solution in all flow regimes. The coupled treatment of particle transport and collision in the evaluation of a time-dependent interface flux function is the key for its cross-scale modeling and ensures a multiple scale nature of the algorithm. The mechanism of flow evolution in different regimes is determined by the ratio between the time step and the local particle collision time. In this paper, the further development of the scheme for a gravitational system is proposed. In order to develop a well-balanced gas-kinetic scheme, the most important ingredient is to take the external force effect into the flux transport across a cell interface. Attempts have been made in the construction of the schemes for the shallow water equations [8] and gas dynamic equations [9, 10, 11]. In this paper, the similar methodology is used in the unified gas kinetic scheme. The scheme can be used to study the multiple scale non-equilibrium flow phenomena under gravitational field, which has never been fully explored before. This paper is organized as following. Section 2 is about the kinetic theory under grav- itational field. Section 3 presents the construction of the unified gas-kinetic scheme for a gravitational system. Section 4 includes numerical examples to demonstrate the performance of the scheme. The last section is the conclusion. 2. Gas kinetic modeling The gas kinetic theory describes the evolution of particle distribution function f(xi,t,ui,ξ) in space and time (xi, t). Here ui =(u,v,w) is particle velocity and ξ is the internal variable for the rotation and vibration. The evolution equation for f in the kinetic scale with the separate modeling of particle transport and collision is the so-called Boltzmann Equation, ft + uifxi + φifui = Q(f, f), where φi is the external forcing term and Q(f, f) is the collision term. Many kinetic models, such as BGK [12], ES-BGK [13], Shakhov [14], and even the full Boltzmann equation [15], can be used in the construction of the unified gas kinetic scheme. Here we use the model equation to explain the principle for the algorithm development. The generalized one-dimensional BGK-type model with the inclusion of external force φx can be written as f + f f + uf + φ f = − , (1) t x x u τ where f + is the equilibrium state, and τ is the collision time. For the BGK equation, f + is exactly the Maxwellian distribution K+1 2 λ 2 2 f + = g = ρ e−λ[(u−U) +ξ ], 0 π 3 where λ = ρ/(2p) and K is the dimension of ξ. For the Shakhov model equation, f + takes the form, c2 f + = g 1+(1 Pr)cq 5 /(5pRT ) , 0 − RT − where c = u U is the peculiar velocity, q is heat flux, and Pr is Prandtl number. The collision term− satisfies the compatibility condition (f + f)ψdΞ=0, − Z 1 2 2 T where ψ = 1, u, 2 (u + ξ ) is a vector of moments for collision invariants, and dΞ= dudξ. The macroscopic conservative flow variables are the moments of the particle distribution function via ρ W = ρU = fψdΞ. ρE Z With a local constant collision timeτ, the integral solution of Eq.(1) can be constructed by the method of characteristics, t 1 ′ f(x,t,u,ξ)= f +(x′, t′,u′,ξ)e−(t−t )/τ dt′ τ tn (2) Z −(t−tn)/τ n n n n + e f0 (x , t ,u ,ξ), ′ ′ ′ 1 ′ 2 ′ ′ where x = x u (t t ) 2 φx(t t ) and u = u φx(t t ) are the trajectories in − − − n − − − physical and phase space, and f0 is the gas distribution function at the beginning of n-th time step.
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